A millisecond pulsar
A millisecond pulsar
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DOI：
10.1038/300615a0
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发表时间：
1982-12
期刊：
影响因子：
64.8
通讯作者：
D. Backer;S. Kulkarni;C. Heiles;Michael M. Davis;W. Goss
中科院分区：
文献类型：
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作者：
D. Backer;S. Kulkarni;C. Heiles;Michael M. Davis;W. Goss
4C21.53的射电性质多年来一直是个谜。首先，该天体显示出81 MHz的行星际微扰（IPS），表明小于1的结构是s，尽管它的银河纬度很低（−0.3°）1。IPS调制在低纬度是罕见的，因为星际角展宽。第二，该光源在十米波长处有一个非常陡峭的（λ v−2）光谱2。这些特性的组合表明，4C21.53要么是一颗未被发现的脉冲星，要么是某类新天体的成员。这个谜团可以通过发现和相关观测到一颗快脉冲星1937+214来解决，它位于狐狸星座，周期为1.558 ms，距离原始脉冲星1919+21的方向只有几度。这种快速脉冲星的存在，既没有新的形成事件的证据，也没有目前的能量损失，这对脉冲星的起源和演化提出了新的问题。
The radio properties of 4C21.53 have been an enigma for many years. First, the object displays interplanetary scintillations (IPS) at 81 MHz, indicating structure smaller than 1 are s, despite its low galactic latitude (−0.3°)1. IPS modulation is rare at low latitudes because of interstellar angular broadening. Second, the source has an extremely steep (∼v−2) spectrum at decametric wavelengths2. This combination of properties suggested that 4C21.53 was either an undetected pulsar or a member of some new class of objects. This puzzle may be resolved by the discovery and related observations of a fast pulsar, 1937+214, with a period of 1.558 ms in the constellation Vulpecula only a few degrees from the direction to the original pulsar, 1919+21. The existence of such a fast pulsar with no evidence either of a new formation event or of present energy losses raises new questions about the origin and evolution of pulsars.